H gamma and H delta Absorption Features in Stars and Stellar Populations
Guy Worthey, & D. L. Ottaviani 1997,
Astrophysical Journal Supplement Series, in press
The catalog consists of 2 files. This is File 1. File 2 contains
average index measurements and atmospheric parameters. Please copy
both of these files when duplicating the catalog.
This computer-readable distribution is meant to summarize ALL of
the data on stellar absorption features published in the "Old Stellar
Populations" series (Faber et al. 1985, Burstein et al. 1986,
Gorgas et al. 1993, hereafter G93, and Worthey et al. 1994), as well
as the current Worthey & Ottaviani paper, which deals with 4 additional
Balmer absorption indices. The main
body of data consists of 21+4 absorption feature indices measured in 460
stars. Additional entries give temperatures, gravities, and metal
abundances for most stars, along with notes on the literature cited or
method used for parameter estimation.
The strength of absorption features in stellar spectra are measured
in terms of "indices" in which a "feature" bandpass is defined
centered on the feature of interest, flanked to the blue and the red
by "pseudocontinuum" bandpasses. The average flux (in wavelength
units) is found for the flanking pseudocontinua, and a straight line
is drawn between the centers of the pseudocontinua. The portion of
this line which lies over the "feature" bandpass is the "continuum"
from which the index is measured by integrating the ratio of
feature/continuum flux over the feature bandpass.
The indices are expressed in two ways. For narrow features
primarily due to atomic species, the index is given as an equivalent
width (EW) in Angstroms. For broader features which measure molecular
line absorption, the index is expressed a flux ratio in magnitudes.
The table below summarizes the 25 index definitions. Note that the
wavelength definitions have been revised from Worthey et al. 1994
through comparison with spectra with better wavelength calibrations.
The listed wavelength definitions are accurate to 0.4 Angstroms.
The CN2 index duplicates the CN1 index too closely to be useful,
except possibly for the study of starburst galaxies. For early-type
galaxies the authors prefer CN1 over CN2, and will adopt the CN1
definition in the future to measure this feature.
Table 1: Index Definitions
------------------------------------------------------------------------Name
Feature Bandpass
Pseudocontinua
Units IDS Error
------------------------------------------------------------------------01 CN 1
4142.125-4177.125
02 CN 2
4142.125-4177.125
4080.125-4117.625
4244.125-4284.125
4083.875-4096.375
4244.125-4284.125
mag
0.021
mag
0.023
03 Ca4227
4222.250-4234.750
4211.000-4219.750
Ang
0.27
4241.000-4251.000
04 G4300
4281.375-4316.375
4266.375-4282.625
Ang
0.39
4318.875-4335.125
05 Fe4383
4369.125-4420.375
4359.125-4370.375
Ang
0.53
4442.875-4455.375
06 Ca4455
4452.125-4474.625
4445.875-4454.625
Ang
0.25
4477.125-4492.125
07 Fe4531
4514.250-4559.250
4504.250-4514.250
Ang
0.42
4560.500-4579.250
08 Fe4668
4634.000-4720.250
4611.500-4630.250
Ang
0.64
4742.750-4756.500
09 H beta
4847.875-4876.625
4827.875-4847.875
Ang
0.22
4876.625-4891.625
10 Fe5015
4977.750-5054.000
4946.500-4977.750
Ang
0.46
5054.000-5065.250
11 Mg 1
5069.125-5134.125
4895.125-4957.625
mag
0.007
5301.125-5366.125
12 Mg 2
5154.125-5196.625
4895.125-4957.625
mag
0.008
5301.125-5366.125
13 Mg b
5160.125-5192.625
5142.625-5161.375
Ang
0.23
5191.375-5206.375
14 Fe5270
5245.650-5285.650
5233.150-5248.150
Ang
0.28
5285.650-5318.150
15 Fe5335
5312.125-5352.125
5304.625-5315.875
Ang
0.26
5353.375-5363.375
16 Fe5406
5387.500-5415.000
5376.250-5387.500
Ang
0.20
5415.000-5425.000
17 Fe5709
5696.625-5720.375
5672.875-5696.625
Ang
0.18
5722.875-5736.625
18 Fe5782
5776.625-5796.625
5765.375-5775.375
Ang
0.20
5797.875-5811.625
19 Na D
5876.875-5909.375
5860.625-5875.625
Ang
0.24
5922.125-5948.125
20 TiO 1
5936.625-5994.125
5816.625-5849.125
mag
0.007
6038.625-6103.625
21 TiO 2
6189.625-6272.125
6066.625-6141.625
mag
0.006
6372.625-6415.125
22 H del_A
4083.500-4122.250
4041.600-4079.750
Ang
0.64
4128.500-4161.000
23 H gam_A
4319.750-4363.500
4283.500-4319.750
Ang
0.48
4367.250-4419.750
24 H del_F
4091.000-4112.250
4057.250-4088.500
Ang
0.40
4114.750-4137.250
25 H gam_F
4331.250-4352.250
4283.500-4319.750
Ang
0.33
4354.750-4384.750
------------------------------------------------------------------------File 2 of this distribution, which contains average index measurements
and atmospheric parameters is organized as follows:
Table 2: File 2 Format
------------------------------------------------------------------------col. bytes format
------------------------------------------------------------------------1
1-10
A10
HD (Henry Draper Catalog) number, if any.
2
11-25
A15
Alternate names for the star. These could be "HR"
3
26-39
A14
numbers (Bright Star Catalog; Hoffleit 1982),
"BD" (Bonner Durchmusterung) numbers, "Gl" numbers
(Nearby Stars; Gleise 1969), cluster names (see
the Appendix of this work), or common names.
This is not a complete cross-reference list.
4-28 40-239 25(F8) Index values, units indicated in the above table.
29
240-249 I10
Effective temperature (source in column 29).
30
250-257 F8
Logarithm of the surface gravity in cm/s^2 (source
in column 30).
31
258-265 F8
[Fe/H] (source in column 31).
32
266-269 I4
Number of observations. This number is the upper
limit
to the actual number of measurements which went into
the index averages, as some portions of some spectra
were missing or otherwise unusable.
33-35 270-281 3(I4) Sources for effective temperature, gravity, and
[Fe/H],
respectively.
36
282-360 A79
Spectral type and comment, if any.
-------------------------------------------------------------------------Here is a sample line, which can be used as a header for File 2:
HD
name1
name2
CN 1
CN 2
Ca4227 G 4300
Fe4383 Ca4455 Fe4531 Fe4668 HB4681 Fe5015
Mg 1
Mg 2
Mg b
Fe5270 Fe5335 Fe5406 Fe5709 Fe5782 Na5895
TiO 1
TiO 2 H del_A
H gam_A H del_F H gam_F
Te
log g [Fe/H] NObs ---notes--Spectral type and comments
-------------------------------------------------------------------------Notes on temperature, gravity, and [Fe/H] (columns 33-35):
The first several are from Table 2 of G93:
Laird (1985)
Cayrel de Strobel et al. (1980)
Wallerstein (1961)
Peterson & Carney (1979)
Johnson et al. (1968)
Peterson (1981)
Yale Bright Star Catalog 4th ed. (Hoffleit 1982)
Dickow et al. (1970)
Clegg et al. (1981)
Cayrel de Strobel et al. (1985)
Gliese (1969)
Computed in G93 using log g from theoretical models (VandenBerg 1983)
versus Te (Veeder 1974) and/or Mbol (Mv from Gliese (1969); BC from
Johnson (1966) versus spectral type).
18. Hearnshaw (1974a,b; 1976a,b)
1.
2.
3.
4.
5.
6.
7.
8.
10.
13.
16.
17.
Most cluster parameters are from Table 4 of G93:
19. [Fe/H] for NGC 188
VandenBerg (1985)
20. [Fe/H] for NGC 7789
[Fe/H]hyades = -0.25, Twarog & Tyson
(1985)
21. [Fe/H] for M67,M71
Burstein et al. (1986)
22. [Fe/H] for Hyades
Boesgaard & Friel, (1990)
23. [Fe/H] for M3,M5,M10,M13,M92 Kraft (1979)
24.
25.
G93
26.
27.
28.
29.
[Fe/H] for Coma cluster
Boesgaard (1987)
Gravities estimated using VandenBerg (1983;1985) isochrones, as in
[Fe/H]o taken from from Faber et al. (1985)
Te, log g, [Fe/H] from Gilroy et al. (1988)
Te, log g, [Fe/H] from Danford & Lea (1981)
Te derived from the relation given by Saxner & Hammarback (1985):
Te = 8065 - 3580(B-V)(1 - 0.196[Fe/H]) 0.30<B-V<0.63
30. Te an average from linear interpolation in Johnson (1966). Both
B-V and R-I were averaged, B-V given twice the weight. For Hyads
vB 64, and vB 73, V-K was used instead of B-V.
31. Te from linear interpolation in Table 3 of Bohm-Vitense (1981),
using the lower temperature scale where appropriate because
it agrees with that of Saxner and Hammarback (1985).
32. Gravities estimated from fundamental parameters Te, M, L. Bolometric
corrections from Johnson (1966), adjusted to VandenBerg's solar BC
of -0.12. Masses estimated using VandenBerg isochrones of ages 0.4
(Coma),
0.7 (Hyades) Gyr.
33. Temperature from the Carney (1983) calibration of THETA-effective
versus V-K. Valid for dwarfs of any metallicity and 4500<Te<7000:
The relation is THETAe = 0.245(V-K) + 0.514. We have found that
this scale doesn't agree at the hot end with Saxner & Hammarback
(1985) or
Bohm-Vitense (1981). We therefore do not use this calibration for
stars
hotter than V-K=1.00. It does agree with Johnson (1966) at the cool
end.
34. Te, log g, [Fe/H] from Adelman & Hill (1987).
35. log g from Stromgren c1 photometry (calibration of Laird 1985).
Mean photometry from the ubvyBeta Photoelectric Photometric Catalog
of Hauck and Mermilliod (1990), computer readable version.
36. Te from fitting functions for (R-I)j in Carney (1983, Appendix I).
37. Straight mean from Cayrel de Strobel et al. (1992).
38. Te from fitting functions for (b-y) in Carney (1983, Appendix I).
40. log g as a function of spectral type, Landolt-Bornstein (1982).
41. Te from linear B-V interpolation in Table 4 of Bohm-Vitense (1981).
42. Te, log g, [Fe/H] from Luck and Bond (1982).
43. log g estimated from color-log g relations defined by Hyades and
Coma clusters
45. For HR 2135, Te is from Underhill et al. (1979). With a
BCv = 0.13 - 0.12 = 0.01 (from Johnson 1966 corrected to
BC(solar)=-0.12), we have V=4.62. With a true distance modulus of
10.57
(1300 pc - Underhill et al.) and an visual extinction = 3*E(B-V) =
3*0.51 = 1.53 (E(B-V) from Greenberg and Chlewicki (1983)),
we have an absolute magnitude of -7.48. Reading from
Figure 1 of Schaller et al. (1992), we estimate a mass of 17
solar masses for this star. The gravity from fundamental relations
is then 2.70.
46. [Fe/H] estimated as in Laird (1985), using the Stromgren m1 index.
47. Average of methods 36 and 38.
48. Te and log g from Ferro, Parrao, and Giridhar (1988).
49. Te and log g estimated from c1 and Beta, from the graphs of Moon and
Dworetsky (1985). For stars later than A0, if the Te obtained
by this method differed by more than 200 K from Bohm-Vitense's
(1981, Table 3) value, the latter was adopted, and log g rederived.
50. [Fe/H] from Cayrel de Strobel et al. (1981).
51. [Fe/H] from Herbig & Wolff (1966).
52. Te and log g from Malagnini & Morossi (1990).
53. [Fe/H] from Gustafsson & Nissen (1972).
54. Te from Gray & Johanson (1991).
55. Parameters from Luck, Bond, & Lambert (1990). Te and log g are
photometrically determined.
56. Te determined by Gulati, Malagnini, & Morossi (1989).
57. Average Te, Mbol, M(evolutionary) and R from Fernley, Skillen, &
Jameson (1989).
58. [Fe/H] from Klochkova & Panchuk (1991). [Fe/H] is solar within the
uncertainties in transforming from the metallicity scale they
employed.
59. [Fe/H] from Hearnshaw (1974a).
60. Te and log L from de Jager et al. (1988). M estimated from
the tracks of Schaller et al. (1992) to derive log g.
(Derived values: HR7678, M=40; HR7977, M=22; HR825, M=18)
61. From Eggen (1991). Te estimated using [c1] and Beta
and the grid of Moon & Dworetsky (1985). log g and P[Fe/H] are
derived by Eggen.
62. Te and log g from Leitherer & Wolf (1984).
63. Te from (B-V)o as a function a spectral type from Landolt-Bornstein
(1982),
converted to Te via Bohm-Vitense (1981).
64. [Fe/H] from Kuroczkin & Wiszniewski (1977).
65. Te from the spectral-type-vs.-Te relation of Ridgway, Joyce, White
and Wing (1980, hereafter RJWW) for M giants.
66. Te from V-K. For giants, calibration is RJWW's, plus one point at
5010 K
from Johnson (1966), plus hotter points from the same reference, but
from the dwarf table. Interpolation was linear. For dwarfs and
subgiants,
Johnson (1966) calibration was used. Input V-K is, in some cases, a
transformation from B-V (see G93 for details).
67. The red dwarfs BD +19 5116 A and B were assigned temperatures
according
to their spectral types from Johnson (1966).
68. Te from Tsuji (1986) based on angular diameters
from Ridgway et al. (1982). [C/H] from the Tsuji analysis. log g = 0
is a
reasonable guess, good to plus or minus 0.5 dex.
69. Gravity estimated in G93 from the Mg2 index.
70.
71.
72.
73.
Leep & Wallerstein (1981).
Brown et al. (1989).
Smith & Lambert (1985).
Gravity for supergiant HR 8752 was taken to be near its evolutionary
value of 0.0, taken from Luck (1975).
74. Some late M giants were assumed to have gravities near 0, which is a
typical value.
75. Effective temperature and bolometric correction from B-V via the
Kurucz (1992) color grids. For the Te/BC derivation
log g was assumed to be 2 for B-V > 0.05, and 3 for
hotter stars. Log g was then calculated from fundamental parameters.
Mass assumed 0.65 Mo, distance moduli from Table 4 of G93 or Table A3
of this work.
76. Metallicity of NGC 6171 = M101 from Zinn & West (1984).
77. Temperature of cool supergiant HR 8752 assigned on the basis of
spectral
type. Johnson (1966). Spectral type is apparently varying with time.
78. Temperatures from Veeder (1974).
79. [Fe/H] an average of Brown et al. (1989) and McWilliam (1990).
80. Parameters from Gratton & Sneden (1991).
81. HR 4365: [Fe/H] and log g from Helfer & Wallerstein (1968).
Hyades [Fe/H] assumed +0.13 (Boesgaard & Friel 1990).
Temperature is an average of that of Helfer & Wallerstein (1968) from
6-color photometry (4253 K) and that deduced from B-V via Johnson
(1966)
and Ridgway et al. (1980) (4450 K). Note that the V-K value quoted
for
this star in Faber et al. (1985) is fictitious (though close
to correct), as the star does not appear in the quoted source
(Johnson et al. 1966). Also note that the temperature for this star
quoted in Cayrel de Strobel et al. (1992) is too low, and
should be THETA = 1.185 (not 1.32).
-------------------------------------------------------------------------References:
Adelman, S.J., & Hill, G. 1987, MNRAS, 226,581
Boesgaard, A.M. 1987, ApJ, 321,967
Boesgaard, A.M., & Friel, E.D., 1990, ApJ, 351,467
Bohm-Vitense, E. 1981, ARAA, 19,295
Brown, J.A., Sneden, C., Lambert, D.L., & Dutchover, E.Jr. 1989, ApJS,
71,293
Burstein, D., Faber, S.M., & Gonzalez, J.J. 1986, AJ, 91,1130
Carney, B.W. 1983, AJ, 88,623
Cayrel de Strobel, G., Bentolila, C., Hauck, B., & Curchod, A. 1980,
A&AS, 41,405
Cayrel de Strobel, G., Knowles, N., Hernandez, G., & Bentolila, C. 1981,
A&A, 94,1
Cayrel de Strobel, G., Bentolila, C., Hauck, B., & Duquennoy, A. 1985,
A&AS, 59,145
Cayrel de Strobel, G., Hauck, B., Francois, P., Thevenin, F., Friel,
E.D.,
Mermilliod, M., & Borde, S. 1992, A&AS, 95,273
Clegg, R.E.S., Lambert, D.C., & Tomkin, J. 1981, ApJ, 250,262
Danford, S.C., & Lea, S.M. 1981, AJ, 86,1909
de Jagar, C., Nieuwenhuijzen, H., & van der Hucht, K.A. 1988, A&AS,
72,259
Dickow, P., Gyldenkerne, K., Hansen, L., Jacobsen, P.-U., Johansen, K.T.,
Kjaergaard, P., & Olsen, E.H. 1970, A&AS, 2,1
Eggen, O.J. 1991, AJ, 102,1826
Faber, S.M., Friel, E.D., Burstein, D., & Gaskell, C.M. 1985, ApJS,
57,711
Fernley, J.A., Skillen, I., & Jameson, R.F. 1989, MNRAS, 237,947
Ferro, A.A., Parrao, L., & Giridhar, S. 1988, PASP, 100,993
Gleise, W. 1969, Catalogue of Nearby Stars, Veroff. Astr. Rechen-Inst.
Heidelberg No. 22
Gilroy, K.K., Sneden, C., Pilachowski, C.A., & Cowan, J.J. 1988, ApJ,
327,298
Gorgas, J., Faber, S.M., Burstein, D., Gonzalez, J.J., Courteau, S., &
Prosser, C. 1993, ApJS, 86,153 (G93)
Gratton, R.G. & Sneden, C. 1991, A&A, 241,501
Gray, D.F. & Johanson, H.L. 1991, PASP, 103,439
Greenberg, J.M., & Chlewicki, G. 1983, ApJ, 272,563
Gulati, R.K., Malagnini, M.L., & Morossi, C. 1989, A&AS, 80,73
Gustafsson, B., & Nissen, P.E. 1972, A&A, 19,261
Hauck, B., & Mermilliod, M. 1990, A&AS, 86,107
Hearnshaw, J.B. 1974a, A&A, 34,263
Hearnshaw, J.B. 1974b, A&A, 36,191
Hearnshaw, J.B. 1976a, A&A, 51,71
Hearnshaw, J.B. 1976b, A&A, 51,85
Helfer, H.L., & Wallerstein, G. 1968, ApJS, 16,1
Herbig, G.H., & Wolff, R.J. 1966, Ann. Astrophys., 29,593
Hoffleit, D. 1982, The Bright Star Catalog, 4th ed., (New Haven:Yale
University Observatory)
Johnson, H.L. 1966, ARA&A, 4,193
Johnson, H.L., MacArthur, J.W., & Mitchell, R.I., 1968, ApJ, 152,465
Johnson, H.L., Mitchell, R.I., Iriarte, B., & Wisniewski, W.Z. 1966,
Comm.
Lunar Planet. Lab., 4,99
Klochkova, V.G., & Panchuk, V.E. 1991, Soviet Astronomy Letters, 17,229
Kraft, R.P., 1979, ARA&A, 17,309
Kuroczkin, D., & Wiszniewski, A., 1977, Acta. Astron., 27,145
Kurucz, R.L. 1992, private communication
Laird, J.B. 1985, ApJS, 57,389
Landolt-Bornstein 1982, Numerical Data and Functional Relationships in
Science and Technology, Vol. 2b, eds. K. Scaifers & H.H. Voigt,
(Springer-Verlag)
Leep, E.M., & Wallerstein, G. 1981, MNRAS, 196,543
Leitherer, C., & Wolf, B. 1984, A&A, 132,151
Luck, R.E. 1975, ApJ, 202,743
Luck, R.E., & Bond, H.E. 1982, ApJ, 263,215
Luck, R.E., Bond, H.E., & Lambert, D.L. 1990, ApJ, 357,188
Malagnini, M.L., & Morossi, C., 1990, A&AS 85,1015
McWilliam, A. 1990, ApJS, 74,1075
Moon, T.T., & Dworetsky, M.M. 1985, MNRAS 217,305
Peterson, R.C. 1981, ApJS, 45,421
Peterson, R.C., & Carney, B.W. 1979, ApJ, 231,762
Ridgway, S.T., Joyce, R.R., White, N.M., & Wing, R.F. 1980, ApJ, 235,126
(RJWW)
Ridgway, S.T., Jacoby, G.H., Joyce, R.R., Siegel, M.J., & Wells, D.C.
1982,
AJ, 87,808
Saxner, M., & Hammarback, G. 1985, A&A, 151,372
Schaller, G., Schaerer, D., Meynet, G., & Maeder, A. 1992, A&AS, 96,269
Smith, V.V., & Lambert, D.L. 1985, ApJ, 294,326
Tsuji, T. 1986, A&A, 156,8
Twarog, B.A., & Tyson, N. 1985, AJ, 90,1247
Underhill, A.B., Divan, L., Prevot-Burnichon, M.-L., & Doazan, V. 1979,
MNRAS, 189,601
VandenBerg, D.A. 1983, ApJS, 51,29
VandenBerg, D.A. 1985, ApJS, 58,711
Veeder, G.J. 1974, AJ, 79,1056
Wallerstein, G. 1961, ApJS, 6,407
Worthey, G., Faber, S.M., Gonzalez, J.J., & Burstein, D. 1994, ApJS,
94,687
Worthey, G., & Ottaviani, D. L. 1997, ApJS, in press
Zinn, R., & West, M. 1984, ApJS, 55,45
--------------------------------------------------------------------------